We present a statistical system that can be used in the study of cluster populations .
The basis of our approach is the construction of synthetic cluster color-magnitude-radius diagrams ( CMRDs ) , which we compare with the observed data using a maximum likelihood calculation .
This approach permits a relatively easy incorporation of incompleteness ( a function of not only magnitude and color , but also radius ) , photometry errors and biases , and a variety of other complex effects into the calculation , instead of the more common procedure of attempting to correct for those effects .

We then apply this procedure to our NGC 3627 data from Paper I .
We find that we are able to successfully model the observed CMRD and constrain a number of parameters of the cluster population .
We measure a power law mass function slope of \alpha = -1.50 \pm 0.07 , and a distribution of core radii centered at r _ { c } = 1.53 \pm 0.15 pc .
Although the extinction distribution is less constrained , we measured a value for the mean extinction consistent with that determined in Paper I from the Cepheids .