Classical gravitational collapse in general relativity generically leads to spacetime singularities, where curvature invariants diverge and predictability breaks down. Non-singular collapse models aim to replace this behavior with a finite-density core and a smooth transition from contraction to expansion, but many such models rely on idealized symmetry assumptions and fail when anisotropy or rotation is introduced. This paper presents a consolidated numerical investigation of anisotropic and rotating non-singular black-hole interior dynamics within the Omegaon Model. Extending earlier homogeneous collapse–bounce solutions, we examine the robustness of the Omegaon bounce mechanism under anisotropy and spin-dependent (Kerr-like) shear, motivated by realistic astrophysical collapse scenarios. An effective shear sector is incorporated phenomenologically into the interior evolution equations, capturing the amplification of anisotropy during collapse, its enhancement with increasing spin, and its rapid decay during post-bounce expansion. The coupled system is evolved numerically across a wide range of shear amplitudes and spin parameters. The results demonstrate that the Omegaon bounce persists robustly in the presence of both anisotropy and rotation. In all cases examined, the system undergoes a smooth transition from contraction to expansion with finite curvature invariants, bounded shear, and localized, transient violation of the null energy condition confined to the immediate bounce phase. No runaway shear growth or destabilization of the background dynamics is observed. These findings establish that the Omegaon non-singular collapse mechanism is not restricted to idealized isotropic models, but remains viable under physically motivated deviations from symmetry. The work provides an essential bridge between homogeneous non-singular collapse and more realistic rotating black-hole interior models, and lays the groundwork for subsequent perturbative and cosmological analyses within the Omegaon framework.