Many Type II-P supernovae (SNe II-P) from the past 25 years have pre-explosion HST imaging in which a red supergiant (RSG) progenitor star is detected, leading to the interpretation that all SNe II-P explode from RSGs in the 8-17 Msun range.  This interpretation is in tension with theoretical models of core-collapse SNe and the Galactic population of RSGs, which suggest that stars in the 17-25 Msun range may produce core-collapse SNe.  I will present pre-explosion HST and Spitzer imaging of the site of the SN II-P 2017eaw in the high SN rate galaxy NGC 6946.  The images span 13 years prior to the discovery of SN 2017eaw.  They indicate that the progenitor system had a significant mid-infrared component to its spectral energy distribution (SED) that was variable by a factor of ~2.  I will present the overall optical to mid-infrared SED of the SN 2017eaw progenitor system and discuss the possibility that it was heavily dust-obscured and therefore exploded from a relatively massive RSG.  I will place this star in the context of other SNe II-P progenitor systems and discuss the possibility that pre-explosion HST imaging alone biases the mass estimates of RSG progenitor systems.  Finally, I will present high-resolution optical spectroscopy of SN 2017eaw obtained immediately after discovery.  These data exhibit narrow, variable, high-ionization features associated with "flash ionized" circumstellar material, further reinforcing the interpretation that SN 2017eaw exploded in a dusty environment.