(Bottom panel) Distribution of Hα luminosities as a function of FUV luminosities corrected for extinction according to the best fitting SED model. Units are erg s^-1. The dashed line shows the linear relation consistent with the distribution for bright clusters. Filled triangles and open circles are for inner and outer disk YSCs, respectively. (Top panel) The same data are shown using small dots together with the average value of log L_Hα (filled squares) in 0.4 wide bins of log L_FUV. The filled circles show the expected values as derived from the simulation of the stochastic IMF for clusters at birth.