Comparison of the distribution of cluster properties for a stochastic IMF (0.08-100 M_⊙) with that derived for Larson’s model (Larson 1982) where the maximum stellar mass varies with the parent cloud mass. As in the previous figures, the cluster mass distribution is a pure power law with α_cl = 1.7, 2.0, and 2.3 and M_clust = 0.03 M_cl. Cluster ages are attributed randomly as described in the text. The bolometric luminosities (bottom) and Hα luminosity (top) were then calculated for the stellar population at the age of each HII region. This figure can be directly compared with Fig. 8.