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The elusive massive black hole (MBH) seeds stand to be revealed by the LaserSpace Antenna Interferometer through mergers. As an aftermath of galaxymergers, MBH coalescence is a vastly multi-scale process connected to galaxyformation. We introduce the "Massive black hole Assembly in Galaxies Informedby Cosmological Simulations" (MAGICS) suite, with galaxy/MBH properties andorbits recovered from large-volume cosmological simulation ASTRID. Thesimulations include subgrid star formation, supernovae feedback, and MBHaccretion/feedback. In this first suite, we extract fifteen representativegalaxy mergers with seed MBHs to examine their dynamics at an improved mass andspatial resolution (by $\sim2000$ and $\sim20$) and follow MBH orbits down to$\sim10\,\text{pc}$. We find that the seed MBH energy loss and orbital decayare largely governed by global torques induced by the galaxy merger process onscales resolvable by cosmological simulations. Specifically, pairs sink quicklyif their orbits shrink rapidly below $1\,\text{kpc}$ during the first$\sim200\,\text{Myr}$ of pairing due to effective energy loss in major galaxymergers, whereas MBHs gaining energy in minor galaxy mergers with head-oncollisions are likely to stall. High initial eccentricities($e_\text{init}>0.5$) and high stellar densities at kpc scales($\rho_\text{star}>0.05\,M_\odot/\text{pc}^3$) also lead to most efficientdecays. $\sim50\%$ high-redshift seed MBH pairs experience consecutive galaxymergers and are more likely to stall at $\sim1\,\text{kpc}$. For a subset ofsystems, we carry out N-Body re-simulations until binary formation and findthat some stalled systems merge at high-z when embedded in sufficient nuclearstar clusters.

MAGICS I. The First Few Orbits Encode the Fate of Seed Massive Black Hole Pairs