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Galaxy clustering measurements can be used to constrain many aspects ofgalaxy evolution, including galaxy host halo masses, satellite quenchingefficiencies, and merger rates. We simulate JWST galaxy clustering measurementsat z$\sim$4$-$10 by utilizing mock galaxy samples produced by an empiricalmodel, the UniverseMachine. We also adopt the survey footprints and typicaldepths of the planned joint NIRCam and NIRSpec Guaranteed Time Observationprogram planned for Cycle 1 to generate realistic JWST survey realizations andto model high-redshift galaxy selection completeness. We find that galaxyclustering will be measured with $\gtrsim$5$\sigma$ significance atz$\sim$4$-$10. Halo mass precisions resulting from Cycle 1 angular clusteringmeasurements will be $\sim$0.2 dex for faint (-18 $\gtrsim$$\mathit{M}_{\mathrm{UV}}^{ }$ $\gtrsim$ -19) galaxies at z$\sim$4$-$10 as wellas $\sim$0.3 dex for bright ($\mathit{M}_{\mathrm{UV}}^{ }$ $\sim$ -20)galaxies at z$\sim$4$-$7. Dedicated spectroscopic follow-up over $\sim$150arcmin$^2$ would improve these precisions by $\sim$0.1 dex by removing chanceprojections and low-redshift contaminants. Future JWST observations willtherefore provide the first constraints on the stellar-halo mass relation inthe epoch of reionization and substantially clarify how this relation evolvesat z$>$4. We also find that $\sim$1000 individual satellites will beidentifiable at z$\sim$4$-$8 with JWST, enabling strong tests of satellitequenching evolution beyond currently available data (z$\lesssim$2). Finally, wefind that JWST observations can measure the evolution of galaxy major mergerpair fractions at z$\sim$4$-$8 with $\sim$0.1$-$0.2 dex uncertainties. Suchmeasurements would help determine the relative role of mergers to the build-upof stellar mass into the epoch of reionization.

Clustering with JWST: Constraining Galaxy Host Halo Masses, Satellite Quenching Efficiencies, and Merger Rates at z=4-10