  We have simulated the Expanded Owens Valley Solar Array (EOVSA) radio images
generated at multiple frequencies from a model solar active region, embedded in
a realistic solar disk model, and explored the resulting datacube for different
spectral analysis schemes to evaluate the potential for realizing one of
EOVSA's most important scientific goals--coronal magnetography. In this paper,
we focus on modeling the gyroresonance and free-free emission from an on-disk
solar active region model with realistic complexities in electron density,
temperature and magnetic field distribution. We compare the magnetic field
parameters extrapolated from the image datacube along each line of sight after
folding through the EOVSA instrumental profile with the original (unfolded)
parameters used in the model. We find that even the most easily automated,
image-based analysis approach (Level 0) provides reasonable quantitative
results, although they are affected by systematic effects due to finite
sampling in the Fourier (uv) plane. Finally, we note the potential for errors
due to misidentified harmonics of the gyrofrequency, and discuss the prospects
for applying a more sophisticated spectrally-based analysis scheme (Level 1) to
resolve the issue in cases where improved uv coverage and spatial resolution
are available.
