  NGC 4945 is a nearby (3.8 Mpc) galaxy hosting a nuclear starburst and Seyfert
Type 2 AGN. We use the Atacama Large Millimeter/submillimeter Array (ALMA) to
image the 93 GHz (3.2 mm) free-free continuum and hydrogen recombination line
emission (H40$\alpha$ and H42$\alpha$) at 2.2 pc (0.12'') resolution. Our
observations reveal 27 bright, compact sources with FWHM sizes of 1.4 - 4.0 pc,
which we identify as candidate super star clusters. Recombination line
emission, tracing the ionizing photon rate of the candidate clusters, is
detected in 15 sources, 6 of which have a significant synchrotron component to
the 93 GHz continuum. Adopting an age of ~5 Myr, the stellar masses implied by
the ionizing photon luminosities are $\log_{10}$($M_{\star}$/M$_{\odot}$)
$\approx$ 4.7 - 6.1. We fit a slope to the cluster mass distribution and find
$\beta = -1.8 \pm 0.4$. The gas masses associated with these clusters, derived
from the dust continuum at 350 GHz, are typically an order of magnitude lower
than the stellar mass. These candidate clusters appear to have already
converted a large fraction of their dense natal material into stars and, given
their small free-fall times of ~0.05 Myr, are surviving an early volatile
phase. We identify a point-like source in 93 GHz continuum emission which is
presumed to be the AGN. We do not detect recombination line emission from the
AGN and place an upper limit on the ionizing photons which leak into the
starburst region of $Q_0 < 10^{52}$ s$^{-1}$.
