High frequency (~10-100 GHz) radio emission from galaxies offers a relatively clean way to quantify current star formation activity. At these frequencies emission is generally optically thin and dominated by free-free radiation, which is directly proportional to the ionizing photon rate of young, massive stars. I will present recent results on the Ka-band (26-40~GHz) emission properties for 10 star-forming regions in the nearby galaxies NGC~6946 observed with the GBT. From a radio spectral decomposition, we find that the 33 GHz flux densities are typically dominated by thermal (free-free) radiation. Treating SFRs derived from the free-free emission as a reference, I will discuss the physical basis and applicability for a number of other extinction-free SFR diagnostics. While the Ka-band appears to provide a reliable measure for the current star formation activity, we also detect excess Ka-band emission for an outer-disk star-forming region relative to what is expected given existing lower frequency radio data. This result is interpreted as the first likely detection of so-called anomalous dust emission outside of the Milky Way. Recent follow-up imaging using CARMA at 92~GHz shows that this excess emission is slightly offset from the individual HII regions identified in higher resolution H-alpha, 8, and 24um maps which make up the star-forming complex. In light of these results, I will discuss the utility of the rest-frame Ka-band for quantifying star formation activity at high-redshifts and how future deep radio surveys at high frequency (i.e., >10 GHz) may help identify variations to the high mass end of the IMF in distant objects.