  To better understand the early stages of massive star cluster evolution we
have obtained J,H,K', and N (10.8 micron) images of the nuclear region of the
starburst galaxy He 2-10. The N-band images were obtained with the Gemini North
telescope and reveal four of the five enshrouded clusters, or "ultradense HII
regions" (UDHIIs), recently discovered in radio maps. None of these sources
appears in either the optical HST images or the near-infrared images. They
comprise about 60% of the total N-band flux from He 2-10 and, we suspect, a
similar fraction of the total far infrared flux measured by IRAS. The inferred
spectra of the UDHIIs are very similar to those of Galactic ultracompact HII
regions and we have modeled the UDHIIs under the assumption that they are
"scaled-up" versions of these objects. The bolometric luminosity of the
brightest UDHII is estimated to be ~2x10^9 L_sun, and the total mass of the
dust and gas is ~10^7 M_sun. The mass of the enshrouded stellar cluster must be
> 2.5x10^6 M_sun and the age must be < 4.8x10^6 yr. All of the stellar clusters
within the UDHIIs must have ages less than about 5x10^6 yr and masses greater
than about 5x10^5 M_sun. The logarithmic ratios of the radio to far infrared
flux densities for the individual UDHIIs, and He 2-10 as a whole, are
significantly larger than the average for normal galaxies, but comparable to
those for ultraluminous infrared galaxies. Large ratios for some starburst
galaxies may indicate that a significant fraction of the far infrared flux
arises from UDHIIs. If all of the far infrared flux from He 2-10 and other
starbursts is produced by heavily obscured regions, the observed correlation
between UV continuum slope and infrared-to-ultraviolet flux ratio in starbursts
cannot be due primarily to UV reprocessing by dust in a foreground screen.
