Nuclear star clusters (NSCs) are dense stellar environments located in the center of most galaxies. NSCs are thought to form through two primary methods: through the inspiral of globular clusters (GCs) to the galactic center due to dynamical friction, and through in situ star formation. Recent observations of dwarf elliptical galaxy UGC 7346 suggest that it might be undergoing NSC formation due to the presence of multiple GCs near its photometric center. We perform direct N-body simulations of nine GCs belonging to UGC 7346’s GC system to investigate whether their eventual infall to the galactic center would result in the formation of an NSC. Our simulations indicate that GCs' inspiral leads to the formation of a central stellar overdensity relative to the background profile of the host galaxy within ∼1.5 Gyr, corresponding to an NSC with a typical mass of (4.1–4.5) × 10⁵ M⊙. Several key structural parameters of the newly formed NSC, including the Sérsic index, effective radius, and central stellar density, lie well within the range observed for NSCs. We also test a hypothetical scenario in which some of the infalling GCs have larger masses (M ∼ 10⁶M⊙), resulting in the formation of a more massive NSC whose mass and size are more consistent with observations. Our results suggest that the inspiral of GCs is a viable channel for assembling a significant mass in the shape of NSCs in the centers of dwarf galaxies and that UGC 7346 will host an NSC at its center in about 2–3 Gyr.