Exoplanet surveys reveal a remarkable diversity in planetary system architectures, ranging from compact super-Earth multiples to widely spaced, eccentric giant planets. This paper presents an integrated framework linking initial protoplanetary disk conditions, planet formation mechanisms, disk-driven migration, and post-disk dynamical evolution to observed orbital configurations. Variations in disk structure, thermodynamics, and angular momentum transport set the initial planetary architecture, while gravitational interactions, resonant coupling, and dynamical instabilities after gas dispersal amplify small differences, producing divergent long-term outcomes. Observed trends in eccentricity, orbital spacing, multiplicity, and resonance occupancy reflect the combined imprint of initial disk conditions and subsequent N-body evolution. We examine observational constraints from transit, radial velocity, and high-resolution millimeter surveys, highlighting selection biases and their implications for theoretical modeling. Our results demonstrate that architectural diversity is an intrinsic outcome of coupled disk and dynamical processes, rather than the result of rare or external perturbations. This framework offers a physically grounded approach for interpreting exoplanet demographics and understanding the dominant processes shaping planetary system evolution.