This paper proposes a structural reinterpretation of globular clusters and cer-tain early black-hole seeds from the perspective of high-density branching in theearly Universe. It does not claim that globular clusters and black holes share aproven common origin, nor does it attempt to replace existing models of globular-cluster formation or black-hole formation. Instead, it suggests that both types ofobjects may be understood as different possible outcomes of early high-density massconcentrations under distinct cooling, fragmentation, and collapse conditions.In the proposed framework, star formation is not treated as the automaticresult of gas concentration. Rather, star formation is understood as a condi-tional pathway that requires sufficient cooling, fragmentation, pressure regulation,angular-momentum redistribution, and a timescale advantage over collective grav-itational collapse. When these conditions succeed, a dense stellar system such asa proto-globular cluster may emerge. When these conditions fail, a high-densitymass concentration may avoid ordinary stellar fragmentation and enter a pre-stellarcollective-collapse pathway that can produce a black-hole seed.This paper distinguishes between post-stellar black holes, which form after stel-lar evolution and collapse, and pre-stellar black-hole seeds, which may form beforeordinary stellar fragmentation becomes dominant. The latter route is not proposedas a universal explanation for all black holes, but as a possible early-universe path-way under special high-density, low-metallicity, inefficient-cooling conditions.The argument connects critical overdensity, fragmentation failure, compactness,cooling time, free-fall time, and a generalized Chandrasekhar-type critical-thresholdlogic. The Chandrasekhar limit is not applied numerically to primordial gas clouds.Rather, its structural lesson is extended: when available support mechanisms canno longer resist gravitational collapse, a transition to a different structural statebecomes possible. In this sense, globular clusters and early black-hole seeds are in-terpreted not as identical objects, but as structurally different outcomes of the samebroader question: did an early high-density mass concentration disperse into manystars, or did collective collapse dominate before stellar fragmentation succeeded?