Several localized outcrops of olivine-enriched bedrock have been previously identified in the Ganges and Eos Chasma area on the eastern end of Valles Marineris with the Thermal Emission Imaging System multispectral images. These outcrops form a layer in the walls of Ganges Chasma and appear to be the remnants of a once continuous unit, which was mapped over ∼100 km. In this study we further characterize the composition (forsterite content of ∼0.68), olivine abundance (10 to >15%), thermal inertia (>600 JK⁻¹ m⁻² s^−1/2, consistent with in-place rocky material), vertical dimension (∼60 to ∼220 m), extent (>1100 km laterally), volume (∼9.9 × 10⁴ km³), dip (∼0.013°NE), and continuity of this layer utilizing Thermal Emission Spectrometer hyperspectral, Thermal Emission Imaging System multispectral, and Mars Orbiter Laser Altimeter elevation data. Morphologic data from high-resolution imagery display a relatively unmantled, rough, and pitted surface associated with the olivine-enriched material, consistent with thermal inertia data. Four possibilities for the origin of the olivine-enriched unit are (1) volcanism associated with tectonic rifting of the Valles Marineris system, (2) a volcaniclastic flow deposit, (3) an intrusive mafic sill, or (4) a discrete episode in Martian history during which flood lavas were erupted onto the surface. The most likely origin is an eruptive event consisting of compositionally uniform flood lavas originating from a primitive mantle source region, possibly associated with the initiation of Tharsis volcanism. This unit is one of the largest continuous compositional units found on Mars and is strikingly similar to other olivine-enriched deposits identified in previous studies where compositional, morphologic, and thermophysical similarities are observed. These similarities may indicate that there was a period in early Martian history, where compositionally uniform and extensive olivine-enriched flood basalts were erupted on the Martian surface.