  This paper presents a comprehensive analysis of the Galactic SNR Kes 17
(G304.6+0.1) with focus on its radio synchrotron emission, environs, and the
factors contributing to the observed gamma rays. The firstly-obtained
integrated radio continuum spectrum from 88 to 8800 MHz yields an index alpha =
-0.488 +/- 0.023 (S_nu $\propto$ nu^alpha), indicative of a linear particle
acceleration process at the shock front. Accounting for the SNR radio shell
size, the distribution of atomic hydrogen (n_H ~ 10 cm^-3), and assuming the
SNR is in the Sedov-Taylor stage of its evolution, we estimate Kes 17 to be
roughly 11 kyr. From 12CO and 13CO (J=1-0) emission-line data as a proxy for
molecular hydrogen we provided the first evidence that the eastern shell of Kes
17 is engulfing a molecular enhancement, with 4.2 x 10^4 M_sun and n ~ 300
cm^-3. Towards the western boundary of Kes 17 there are not CO signatures above
3 sigma, despite previously reported infrared observations have revealed
shocked molecular gas at that location. This suggests the existence of a
CO-dark interacting molecular gas, a phenomenon also recorded in other Galactic
SNRs (e.g. CTB 37A and RX J1713.7-3946). Additionally, by analysing ~14.5 yr of
data from Fermi-LAT, we determined a power-law photon index in the 0.3-300 GeV
range of Gamma = 2.39 +/- 0.04^+0.063_-0.114 (+/-stat +/-syst) in agreement
with prior studies. The energy flux turns out to be (2.98 +/- 0.14) x 10^-11
erg cm-2 s-1 implying a luminosity (2.22 +/- 0.45) x 10^35 erg s-1 at ~8 kpc.
Finally, we successfully modelled the multiwavelength SED by incorporating the
improved radio synchrotron spectrum and the new gamma-ray measurements. Our
analysis indicates that the observed GeV flux most likely originates from the
interaction of Kes 17 with western ''dark'' CO zone with a proton density n_p ~
400 cm-3.
