SN 2014C was originally classified as a Type Ib supernova, but at phase {phi}=127d, 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}=947-2494d post-explosion. We address the evolution of the broadened H{alpha} emission line, as well as broad [OIII] emission and other lines. We also conduct a parallel analysis of all publicly available multiwavelength data. From our spectra, we find a nearly constant H{alpha} FWHM velocity width of ~2000km/s that is significantly lower than that of other broadened atomic transitions (~3000-7000km/s) present in our spectra ([OI]{lambda}6300; [OIII]{lambda}{lambda}4959,5007; HeI{lambda}7065; [CaII]{lambda}{lambda}7291,7324). The late radio data demand a fast forward shock (~10000km/s at {phi}=1700d) 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.