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The physical properties of star cluster populations offer valuable insightsinto their birth, evolution, and disruption. However, individual stars inclusters beyond the nearest neighbours of the Milky Way are unresolved, forcinganalyses of star cluster demographics to rely on integrated light, a processthat is fraught with uncertainty. Here infer the demographics of the clusterpopulation in the benchmark galaxy NGC 628 using data from the LegacyExtra-galactic UV Survey (LEGUS) coupled to a novel Bayesian forward-modellingtechnique. Our method allows analysis of a total of 1178 clusters in the LEGUScatalogue, roughly a factor of 4 more than previous studies that requiredsevere completeness cuts to the data. Our results indicate that the clustermass function is truncated at $\sim 10^4$ $ \mathrm{M}_{\odot}$, consistentwith proposed relations between truncation mass and star formation surfacedensity. We find that cluster disruption begins early, $\sim 10$ Myr afterformation, but that it is relatively mild, with clusters requiring on average$2-3$ times their present age to disrupt; we do not find any evidence for massdependent disruption. We also do not find convincing evidence for any radialvariations in these conclusions, though we find suggestive hints that innergalaxy clusters may be more prone to disruption. Confirming or refuting thesehints will require future observations to increase the sample size of outergalaxy clusters.

Cluster Population Demographics in NGC 628 Derived from Stochastic Population Synthesis Models