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The morphology of HII regions around young star clusters provides insightinto the timescales and physical processes that clear a cluster's natal gas. Westudy ~700 young clusters (<10Myr) in three nearby spiral galaxies (NGC 7793,NGC 4395, and NGC 1313) using Hubble Space Telescope (HST) imaging from LEGUS(Legacy ExtraGalactic Ultraviolet Survey). Clusters are classified by theirH$\alpha$ morphology (concentrated, partially exposed, no-emission) and whetherthey have neighboring clusters (which could affect the clearing timescales).Through visual inspection of the HST images, and analysis of ages, reddenings,and stellar masses from spectral energy distributions fitting, together withthe (U-B), (V-I) colors, we find: 1) the median ages indicate a progressionfrom concentrated (~3 Myr), to partially exposed (~4 Myr), to no H$\alpha$emission (>5Myr), consistent with the expected temporal evolution of HIIregions and previous results. However, 2) similarities in the age distributionsfor clusters with concentrated and partially exposed H$\alpha$ morphologiesimply a short timescale for gas clearing (<1Myr). 3) our cluster sample'smedian mass is ~1000 M, and a significant fraction (~20%) contain one or morebright red sources (presumably supergiants), which can mimic reddening effects.Finally, 4) the median E(B-V) values for clusters with concentrated H$\alpha$and those without H$\alpha$ emission appear to be more similar than expected(~0.18 vs. ~0.14, respectively), but when accounting for stochastic effects,clusters without H$\alpha$ emission are less reddened. To mitigate stochasticeffects, we experiment with synthesizing more massive clusters by stackingfluxes of clusters within each H$\alpha$ morphological class. Compositeisolated clusters also reveal a color and age progression for H$\alpha$morphological classes, consistent with analysis of the individual clusters.

H$\alpha$ Morphologies of Star Clusters: A LEGUS study of HII region evolution timescales and stochasticity in low mass clusters