We present an evaluative study of some current methods utilized in the analysis of infrared (IR) observatinons of star-forming regions. A series of self-consistent radiative transfer models are constructed, with the outputs analysed using these methods to infer source properties such as dust temperature, mass, opacity function, and density distribution. Any discrepancies between the inferred and model quantities can be attributed to the analysis methods. The range of validity of most methods is smaller than expected, due to two effects: (1) limited applicability of the Rayleigh-Jeans limit except to very long wavelengths, and (2) significant errors in the isothermal approximation, even when temperature variations are less than 2 K over 90% of the region. Still, an accurate mean dust temperature can be found using a modified Wien's law. This temperature can yield dust masses to within 10-25% -- much better than masses inferred from the integrated luminosity. Using long wavelengths (greater than 1000 - 2000 microns), the opacity index can be determined from the far-IR spectrum to within 20%. Fitting the spectrum yields better results. The desnity distribution can be somewhat constrained by fitting the surface brightness, for well-resolved sources. Better results are found by fitting the flux spectrum with detailed models.