  Kes 69 is a mixed-morphology (MM) supernova remnant (SNR) that is known to be
interacting with molecular clouds based on 1720 MHz hydroxyl (OH) maser
emission observations in the northeastern and southeastern regions. We present
an investigation of Kes 69 using $\sim$67 ks Suzaku observation. The X-ray
spectrum of the whole SNR is well fitted by a non-equilibrium ionization model
with an electron temperature of $kT_{\rm e}$ $\sim$ 2.5 keV, ionization
time-scale of $\tau$ $\sim$ 4.1$\times10^{10}$ cm$^{-3}$ s and absorbing column
density of $N_{\rm H}$ $\sim$ 3.1$\times10^{22}$ cm$^{-2}$. We clearly detected
the Fe-K$\alpha$ line at $\sim$6.5 keV in the spectra. The plasma shows
slightly enhanced abundances of Mg, Si, S and Fe indicating that the plasma is
likely to be of ejecta origin. We find no significant feature of a recombining
plasma in this SNR. In order to characterize radial variations in the X-ray
spectral parameters, we also analyze annular regions in the remnant. We
investigate the explosive origin of Kes 69 and favor the core-collapse origin.
Additionally, we report a lack of significant gamma-ray emission from Kes 69,
after analyzing the GeV gamma-ray data taken for about 9 years by the Large
Area Telescope on board Fermi. Finally, we discuss the properties of Kes 69 in
the context of other interacting MM SNRs.
