Eccentric binary black holes (BBHs) formed through dynamical interactions can significantly contribute to gravitational wave (GW) detections. In this work, we present a simulated catalog of dynamically formed, stellar-mass BBHs in the local universe, incorporating contributions from the Galactic field (flyby interactions), Galactic nucleus (eccentric Kozai-Lidov evolution), and globular clusters ($N$-body interactions). Our results predict a wide, highly eccentric BBH population in the Milky Way, with source counts of $\sim 25$, 9, 3, 1, and $<1$ for a 4-year LISA mission ($\sim 36$, 13, 5, 2, and 1 for a 10-year extended mission), for $\mathrm{SNR}>1$, 3, 8, 20, and 50, respectively. Extending this model to cosmological populations, we show that different dynamical channels can produce distinct eccentricity distributions in the LVK band and can contribute hundreds of additional low-SNR mHz sources. Specifically, our model yields a merger rate of $\mathrm{\Gamma }\sim 9{\mathrm{Gpc}}^{-3}{\mathrm{yr}}^{-1}$ and $\sim 150$ extragalactic mHz BBHs with $\mathrm{SNR}>1$. However, due to the lower mass and weaker GW signals of stellar-mass BBHs, this number declines sharply at higher detection thresholds (e.g., $\sim 1$ for $\mathrm{SNR}>8$). We further highlight the impact of eccentric BBH signals on the LISA global fit, showing that their individual harmonics can be independently detected in the Milky Way, and may mimic circular binaries with systematically biased chirp masses. Lastly, we show that post-Newtonian waveforms converge reliably for eccentric BBHs with masses of $\lesssim {10}^3{M}_{\odot }$ in the mHz band. Overall, eccentric BBHs represent a prevalent and promising target for future space-based GW observatories.

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• General relativity
• Gravitational wave detection
• Gravitational wave sources
• Gravitational waves