  We survey the young star cluster population in the dwarf galaxy NGC4449 with
the goal of investigating how stellar feedback may depend on the clusters'
properties. Using Ultraviolet(UV)-optical-NearIR(NIR) photometry obtained from
the Hubble Space Telescope, we have recovered 99 compact sources exhibiting
emission in the Pa$\beta$ hydrogen recombination line. Our analysis reveals
these sources possess masses $10^{2}<M_{\odot}<10^{5}$, ages 1-20 Myr, and
color excess E(B - V) in the range 0-1.4. After selecting clusters with mass
above 3,000M$_{\odot}$ to mitigate stochastic sampling of the stellar initial
mass function, we find that our IR-selected clusters have a median mass of
$\sim$7$\times{10^{3}\text{ M}_{\odot}}$ and remain embedded in their
surrounding gas and dust for 5-6 Myr. In contrast, line-emitting sources
selected from existing UV/optically catalogs have a median mass of
$\sim$3.5$\times{10^{4}\text{ M}_{\odot}}$ and have cleared their surroundings
by 4 Myr. We further find that the environment in NGC4449 is too low pressure
to drive these differences. We interpret these findings as evidence that the
clearing timescale from pre-supernova and supernova feedback is cluster
mass-dependent. Even in clusters with mass$\sim$7,000~M$_{\odot}$, stochastic
sampling of the upper end of the stellar initial mass function is present,
randomly decreasing the number of massive stars available to inject energy and
momentum into the surrounding medium. This effect may increase the clearing
timescales in these clusters by decreasing the effectiveness of both
pre-supernova and supernova feedback; neither models nor observations have so
far explored such dependence explicitly. Future studies and observations with,
e.g., the JWST, will fill this gap.
