Dust devil tracks are abundant on Mars, and can significantly change the regional surface albedo, possibly altering regional-scale atmospheric circulations. However, little is understood about the formation of these features, besides their correlation with dust devils. The Mars Regional Atmospheric Modeling System (MRAMS) is used here to explicitly simulate the formation of a dust devil track. The example dust devil (200 m in diameter) studied in detail here generates a track approximately 1.5 km long, 75 m wide, and 1--8 ¿m in depth, which compares well with observed real-world tracks. Valuable insight is gleaned from the study of the formation of this simulated track, which may be used to better interpret the linkage between observed dust devil tracks and the atmospheric and surface conditions that spawned them.