  The nearby SN 2017eaw is a Type II-P (``plateau') supernova showing
early-time, moderate CSM interaction. We present a comprehensive study of this
SN including the analysis of high-quality optical photometry and spectroscopy
covering the very early epochs up to the nebular phase, as well as near-UV and
near-infrared spectra, and early-time X-ray and radio data. The combined data
of SNe 2017eaw and 2004et allow us to get an improved distance to the host
galaxy, NGC 6946, as $D \sim 6.85$ $\pm 0.63$ Mpc; this fits in recent
independent results on the distance of the host and disfavors the previously
derived (30% shorter) distances based on SN 2004et. From modeling the nebular
spectra and the quasi-bolometric light curve, we estimate the progenitor mass
and some basic physical parameters for the explosion and the ejecta. Our
results agree well with previous reports on a RSG progenitor star with a mass
of $\sim15-16$ M$_\odot$. Our estimation on the pre-explosion mass-loss rate
($\dot{M} \sim3 \times 10^{-7} -$ $1\times 10^{-6} M_{\odot}$ yr$^{-1}$) agrees
well with previous results based on the opacity of the dust shell enshrouding
the progenitor, but it is orders of magnitude lower than previous estimates
based on general light-curve modeling of Type II-P SNe. Combining late-time
optical and mid-infrared data, a clear excess at 4.5 $\mu$m can be seen,
supporting the previous statements on the (moderate) dust formation in the
vicinity of SN 2017eaw.
