M dwarfs spend approximately 1 Gyr settling onto the main sequence, compared to the ~10 Myr for G dwarfs. This pre-main sequence phase is characterized by high stellar luminosities, thus any planets in the main sequence habitable zone (HZ) of an M dwarf are subject to extreme levels of insolation during their early evolution that may cause substantial loss of surface water to space. Traditional habitability models have focused on stellar insolation as the most important factor driving ocean loss. However, other factors that might be significant include orbital parameters and tidal heating. Terrestrial planets orbiting in the HZ around red dwarf stars have very short orbital periods relative to the Earth and thus are subjected to significant tidal effects. When planets possess a non-zero eccentricity, one of these effects is significant internal heating from tidal dissipation, which could equal or exceed the tidal heating of Jupiter’s moon Io. Tidal heating can provide sufficient surface heat flux to trigger a thermal greenhouse runaway that manifests in large water loss and oxygen buildup, even if early insolation is reduced. The habitability of rocky worlds is not well understood, and consequently, the impact of tidal heating rates on these planets needs further exploration. Utilizing the virtual planet simulator VPlanet, this study explores how non-zero eccentricities and associated tidal heating affect the surface water loss experienced by Earth-mass terrestrial planets in or near the habitable zones of M dwarf stars during the first Gyr after formation. This work was partially supported by the NSF funded Stanford Undergraduate Research in Geosciences and Engineering (SURGE) program.