  Multi-wavelength images from the Hubble Space Telescope covering the
wavelength range 0.27-1.6 $\mu$m show that the central area of the nearby dwarf
galaxy NGC4449 contains several tens of compact sources that are emitting in
the hydrogen recombination line Pa$\beta$ (1.2818 $\mu$m) but are only
marginally detected in H$\alpha$ (0.6563 $\mu$m) and undetected at wavelengths
$\lambda\le$0.55 $\mu$m. An analysis of the spectral energy distributions
(SEDs) of these sources indicates that they are likely relatively young star
clusters heavily attenuated by dust. The selection function used to identify
the sources prevents meaningful statistical analyses of their age, mass, and
dust extinction distributions. However, these cluster candidates have ages
$\sim$5-6 Myr and A$_V>$6 mag, according to their SED fits, and are extremely
compact, with typical deconvolved radii of 1 pc. The dusty clusters are located
at the periphery of dark clouds within the galaxy and appear to be partially
embedded. Density and pressure considerations indicate that the HII regions
surrounding these clusters may be stalled, and that pre-supernova feedback has
not been able to clear the clusters of their natal cocoons. These findings are
in potential tension with existing models that regulate star formation with
pre-supernova feedback, since pre-supernova feedback acts on short timescales,
$\lesssim$4 Myr, for a standard Stellar Initial Mass function. The existence of
a population of dusty star clusters with ages $>$4 Myr, if confirmed by future
observations, paints a more complex picture for the role of stellar feedback in
controlling star formation.
