We propose that Mars originated as a tidally locked moon of Venus, formed from debris ejected during a giant impact that reversed Venus’ rotation approximately 4.5 billion years ago. This hypothesis offers a unified explanation for several of Mars’ most enigmatic features: its anomalously small mass for its orbital position, its extreme hemispheric dichotomy, and its apparent displacement from standard planetary formation models. The proposed impact would have generated a substantial debris field, analogous to the Earth–Moon–forming event. Mars subsequently coalesced from this material in close orbit around Venus, becoming tidally locked. The hemisphere facing Venus—now Mars’ northern lowlands—experienced intense tidal heating, while the opposite hemisphere—now the southern highlands—remained relatively stable. This differential heating produced the dramatic crustal thickness variations and geological contrasts observed today. Due to the large mass ratio between Mars and Venus (0.13), tidal evolution proceeded rapidly. Within 500–1000 million years, Mars spiraled outward and escaped Venus’ gravitational influence, eventually stabilizing in its current heliocentric orbit. The hemispheric dichotomy thus represents a fossil record of Mars’ tidally locked phase. This hypothesis makes several testable predictions: isotopic similarities between Venus and Mars, asymmetric crustal structures consistent with tidal heating, and geochemical signatures of thermal fractiMaronation. Validation would require coordinated sample return missions, hemispheric geophysical mapping, and comparative analysis with the Earth–Moon system. If confirmed, this paradigm would fundamentally reshape our understanding of terrestrial planet formation and the role of giant impacts in sculpting planetary systems.