  We present a new catalog and results for the cluster system of the starburst
galaxy NGC 4449 based on multi-band imaging observations taken as part of the
LEGUS and Halpha-LEGUS surveys. We improve the spectral energy fitting method
used to estimate cluster ages and find that the results, particularly for older
clusters, are in better agreement with those from spectroscopy. The inclusion
of Halpha measurements, the role of stochasticity for low mass clusters, the
assumptions about reddening, and the choices of SSP model and metallicity all
have important impacts on the age-dating of clusters. A comparison with ages
derived from stellar color-magnitude diagrams for partially resolved clusters
shows reasonable agreement, but large scatter in some cases. The fraction of
light found in clusters relative to the total light (i.e., T_L) in the U, B,
and V filters in 25 different ~kpc-size regions throughout NGC 4449 correlates
with both the specific Region Luminosity, R_L, and the dominant age of the
underlying stellar population in each region. The observed cluster age
distribution is found to decline over time as dN/dt ~ t^g, with g=-0.85+/-0.15,
independent of cluster mass, and is consistent with strong, early cluster
disruption. The mass functions of the clusters can be described by a power law
with dN/dM ~ M^b and b=-1.86+/-0.2, independent of cluster age. The mass and
age distributions are quite resilient to differences in age-dating methods.
There is tentative evidence for a factor of 2-3 enhancement in both the star
and cluster formation rate ~100 - 300 Myr ago, indicating that cluster
formation tracks star formation generally. The enhancement is probably
associated with an earlier interaction event.
