In the past years, multiple detections of methane in Mars' atmosphere have raised numerous questions about its potential sources. Independently of methane formation mechanism(s), CH4 produced in the past or at the present day could be stored in subsurface reservoirs such as clathrate hydrates. In this work, global maps of stability depth of CH4-rich clathrate hydrates in the martian soil are obtained by including in the subsurface model a top layer with thermal properties that fit with the thermal inertia derived from MGS TES observations (Putzig and Mellon, 2007) and by taking into account the spatial variations of the surface heat flow (Parro et al., 2017). In addition, the spatial distribution of stable methane clathrates is investigated in the presence of eutectic NaCl and CaCl2 brines. The influence of gas phase composition on clathrate stability and on guests abundance is also examined by considering the CO2-CH4-N2 and CO2CH4-H2 mixtures.On present-day Mars, the stability conditions of CH4-rich clathrates are met at a depth of a few meters in high latitude regions and at a few tens of meters deep at the equator. The top of their stability zone is the deepest (~68 m) in regions where methane has been locally reported, especially in the area observed by Mumma et al. (2009). It is also in that particular region that the methane clathrate stability zone is the least extended in the martian subsurface, its base reaching ~8 km deep in the presence of pure water. This depth can even be 4 times shallower if methane clathrates form in the presence of eutectic CaCl2 brine. Moreover, the incorporation of nitrogen and hydrogen in mixed CO2-CH4 clathrates allows a better trapping of methane but their presence increases the formation pressure and therefore their stability depth.