  Next generation ground-based gravitational wave (GW) detectors are expected
to detect $\sim 10^4 \mbox{-} 10^5$ binary black holes (BBHs) per year.
Understanding the formation pathways of these binaries is an open question.
Orbital eccentricity can be used to distinguish between the formation channels
of compact binaries, as different formation channels are expected to yield
distinct eccentricity distributions. Due to the rapid decay of eccentricity
caused by the emission of GWs, measuring smaller values of eccentricity poses a
challenge for current GW detectors due to their limited sensitivity. In this
study, we explore the potential of next generation GW detectors such as
Voyager, Cosmic Explorer (CE), and Einstein Telescope (ET) to resolve the
eccentricity of BBH systems. Considering a GWTC-3 like population of BBHs and
assuming some fiducial eccentricity distributions as well as an astrophysically
motivated eccentricity distribution (Zevin et $al.$ (2021)), we calculate the
fraction of detected binaries that can be confidently distinguished as
eccentric. We find that for Zevin eccentricity distribution, Voyager, CE, and
ET can confidently measure the non-zero eccentricity for $\sim 3\%$, $9\%$, and
$13\%$ of the detected BBHs, respectively. In addition to the fraction of
resolvable eccentric binaries, our findings indicate that Voyager, CE, and ET
require typical minimum eccentricities $\gtrsim 0.02$, $5\times 10^{-3}$, and
$10^{-3}$ at $10$ Hz GW frequency, respectively, to identify a BBH system as
eccentric. The better low-frequency sensitivity of ET significantly enhances
its capacity to accurately measure eccentricity.
