  SN 2014C was originally classified as a Type Ib supernova, but at phase
{\phi} = 127 d post-explosion strong H{\alpha} emission was observed. SN 2014C
has since been observed in radio, infrared, optical and X-ray bands. Here we
present new optical spectroscopic and photometric data spanning {\phi} = 947 -
2494 d post-explosion. We address the evolution of the broadened H{\alpha}
emission line, as well as broad [O III] emission and other lines. We also
conduct a parallel analysis of all publicly available multi-wavelength data.
From our spectra, we find a nearly constant H{\alpha} FWHM velocity width of
{\sim}2000 km/s that is significantly lower than that of other broadened atomic
transitions ({\sim}3000 - 7000 km/s) present in our spectra ([O I]
{\lambda}6300; [O III] {\lambda}{\lambda}4959,5007; He I {\lambda}7065; [Ca II]
{\lambda}{\lambda}7291,7324). The late radio data demand a fast forward shock
({\sim}10,000 km/s at {\phi} = 1700 d) in rarified matter that contrasts with
the modest velocity of the H{\alpha}. We propose that the infrared flux
originates from a toroidal-like structure of hydrogen surrounding the
progenitor system, while later emission at other wavelengths (radio, X-ray)
likely originates predominantly from the reverse shock in the ejecta and the
forward shock in the quasi-spherical progenitor He wind. We propose that the
H{\alpha} emission arises in the boundary layer between the ejecta and torus.
We also consider the possible roles of a pulsar and a binary companion.
