  In a recent paper, we determined the measurement accuracy of physical
parameters for eccentric, precessing, non-spinning, inspiraling, stellar-mass
black hole - black hole (BH-BH) binaries for the upcoming second-generation
LIGO/VIRGO/KAGRA detector network at design sensitivity using the Fisher matrix
method. Here we extend that study to a wide range of binary masses including
neutron star - neutron star (NS-NS), NS-BH, and BH-BH binaries with BH masses
up to $110 \, M_{\odot}$. The measurement error of eccentricity $e_{10 \,\rm
Hz}$ at a gravitational-wave (GW) frequency of $10 \, {\rm Hz}$ is in the range
$(10^{-4}-10^{-3}) \times (D_L/ 100\,\rm Mpc)$ for NS-NS, NS-BH, and BH-BH
binaries at a luminosity distance of $D_L$ if $e_{10 \,\rm Hz} \gtrsim 0.1 $.
For events with masses and distances similar to the detected 10 GW transients,
we show that nonzero orbital eccentricities may be detected if $0.081 \lesssim
e_{10 \,\rm Hz}$. Consequently, the LIGO/VIRGO/KAGRA detector network at design
sensitivity will have the capability to distinguish between eccentric waveforms
and circular waveforms. In comparison to circular inspirals, we find that the
chirp mass measurement precision can improve by up to a factor of $\sim 20$ and
$\sim 50-100$ for NS-NS and NS-BH binaries with BH companion masses $\lesssim
40 \, M_{\odot}$, respectively. The identification of eccentric sources may
give information on their astrophysical origin; it would indicate merging
binaries in triple or higher multiplicity systems or dynamically formed
binaries in dense stellar systems such as globular clusters or galactic nuclei.
