Conditions of crater saturation and equilibrium have been simulated with a Monte Carlo computer program which utilizes a generating function of the form N=b⋅D-1. The following conclusions have been deduced from the results of the model: (1) saturation and equilibrium for large craters occur at crater densities substantially greater than those observed on the moon, Mars, and Mercury, an indication that the observed populations are essentially production populations; (2) generating functions with a>2 lead to final crater populations with a=2; (3) generating functions with 2?a?1.5 lead to crater populations with the parameter a approaching 1.0; and (4) changes in the slope of crater populations occur gradually and over a wide interval of crater densities and diameters as saturation is approached, not, as is often visualized, instantaneously upon rearching a critical crater density.