Molecular clouds are often modeled as isothermal, supersonic turbulent-media, within which stars form in regions whose local free-fall times are shorter than the Eddy turnover timescale. While the evolution of the density distribution in such media is correlated at short times, I show using numerical simulations that for dense regions and moderate timescales, the evolution of the density distribution is well modeled as a Markov Process. Furthermore, as the a steady-state density probability density function of an isothermal turbulent is approximately a log-normal distribution, this evolution can be modeled as an Ornstein-Uhlenbeck process, which takes on a very simple form with only 1 key parameter, the rate of change of the log density. We measure this parameter as a function of Mach number, use it to construct a model of star formation with a first order differential equation, and compare it to the results of full turbulent simulations with gravity.