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We present multi-wavelength images observed with SOFIA-FORCAST from $\sim$10to 40 $\mu$m of seven high luminosity massive protostars, as part of the SOFIAMassive (SOMA) Star Formation Survey. Source morphologies at these wavelengthsappear to be influenced by outflow cavities and extinction from dense gassurrounding the protostars. Using these images, we build spectral energydistributions (SEDs) of the protostars, also including archival data fromSpitzer, Herschel and other facilities. Radiative transfer (RT) models of Zhang& Tan (2018), based on Turbulent Core Accretion theory, are then fit to theSEDs to estimate key properties of the protostars. Considering the best fivemodels fit to each source, the protostars have masses $m_{*} \sim 12-64 \:M_{\odot}$ accreting at rates of $\dot{m}_{*} \sim 10^{-4}-10^{-3} \: M_{\odot}\: \rm yr^{-1}$ inside cores of initial masses $M_{c} \sim 100-500 \:M_{\odot}$ embedded in clumps with mass surface densities $\Sigma_{\rm cl} \sim0.1-3 \: \rm g \: cm^{-2}$ and span a luminosity range of $10^{4} -10^{6} \:L_{\odot}$. Compared with the first eight protostars in Paper I, the sourcesanalyzed here are more luminous, and thus likely to be more massive protostars.They are often in a clustered environment or have a companion protostarrelatively nearby. From the range of parameter space of the models, we do notsee any evidence that $\Sigma_{\rm cl}$ needs to be high to form these massivestars. For most sources the RT models provide reasonable fits to the SEDs,though the cold clump material often influences the long wavelength fitting.However, for sources in very clustered environments, the model SEDs may not besuch a good description of the data, indicating potential limitations of themodels for these regions.

The SOFIA Massive (SOMA) Star Formation Survey. II. High Luminosity Protostars