  The Kepler mission has provided exquisite data to perform an ensemble
asteroseismic analysis on evolved stars. In this work we systematically
characterize solar-like oscillations and granulation for 16,094 oscillating red
giants, using end-of-mission long-cadence data. We produced a homogeneous
catalog of the frequency of maximum power (typical uncertainty
$\sigma_{\nu_{\rm max}}$=1.6\%), the mean large frequency separation
($\sigma_{\Delta\nu}$=0.6\%), oscillation amplitude ($\sigma_{\rm A}$=4.7\%),
granulation power ($\sigma_{\rm gran}$=8.6\%), power excess width ($\sigma_{\rm
width}$=8.8\%), seismically-derived stellar mass ($\sigma_{\rm M}$=7.8\%),
radius ($\sigma_{\rm R}$=2.9\%), and thus surface gravity ($\sigma_{\log
g}$=0.01 dex). Thanks to the large red giant sample, we confirm that
red-giant-branch (RGB) and helium-core-burning (HeB) stars collectively differ
in the distribution of oscillation amplitude, granulation power, and width of
power excess, which is mainly due to the mass difference. The distribution of
oscillation amplitudes shows an extremely sharp upper edge at fixed $\nu_{\rm
max}$, which might hold clues to understand the excitation and damping
mechanisms of the oscillation modes. We find both oscillation amplitude and
granulation power depend on metallicity, causing a spread of 15\% in
oscillation amplitudes and a spread of 25\% in granulation power from
[Fe/H]=-0.7 to 0.5 dex. Our asteroseismic stellar properties can be used as
reliable distance indicators and age proxies for mapping and dating galactic
stellar populations observed by Kepler. They will also provide an excellent
opportunity to test asteroseismology using Gaia parallaxes, and lift
degeneracies in deriving atmospheric parameters in large spectroscopic surveys
such as APOGEE and LAMOST.
