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(Abridged) I present a predictive analysis for the behavior of the FIR--radiocorrelation as a function of redshift in light of the deep radio continuumsurveys which may become possible using the SKA. To keep a fixed ratio betweenthe FIR and predominantly non-thermal radio continuum emission of a normalstar-forming galaxy requires a nearly constant ratio between galaxy magneticfield and radiation field energy densities. While the additional term of IClosses off of the cosmic microwave background (CMB) is negligible in the localUniverse, the rapid increase in the strength of the CMB energy density (i.e.$\sim(1+z)^{4})$ suggests that evolution in the FIR-radio correlation shouldoccur with infrared (IR; $8-1000 \micron$)/radio ratios increasing withredshift. At present, observations do not show such a trend with redshift;$z\sim6$ radio-quiet QSOs appear to lie on the local FIR-radio correlationwhile a sample of $z\sim4.4$ and $z\sim2.2$ SMGs exhibit ratios that are afactor of $\sim$2.5 {\it below} the canonical value. I also derive a 5$\sigma$point-source sensitivity goal of $\approx$20 nJy (i.e. $\sigma_{\rm RMS} \sim4$ nJy) requiring that the SKA specified be $A_{\rm eff}/T_{\rm sys}\approx15000$ m$^{2}$ K$^{-1}$; achieving this sensitivity should enable the detectionof galaxies forming stars at a rate of $\ga25 M_{\sun} {\rm yr}^{-1}$, at allredshifts if present. By taking advantage of the fact that the non-thermalcomponent of a galaxy's radio continuum emission will be quickly suppressed byIC losses off of the CMB, leaving only the thermal (free-free) component, Iargue that deep radio continuum surveys at frequencies $\ga$10 GHz may prove tobe the best probe for characterizing the high-$z$ star formation history of theUniverse unbiased by dust.

The Far-Infrared--Radio Correlation at High Redshifts: Physical Considerations and Prospects for the Square Kilometer Array