  All 4 giant planets in the Solar System host systems of multiple moons,
whereas the terrestrial planets only host up to 2 moons. The Earth can capture
small asteroids as temporary satellites, which begs the question as to how many
moons could stably orbit the Earth, or an Earth-mass exoplanet. We perform a
series of N-body simulations of closely-spaced equal mass moons in nested
orbits around an Earth-mass planet orbiting a Sun-like star. The innermost moon
begins near the host planets Roche radius, and the system is packed until the
outermost moon begins near the stability limit for single moons. The initial
spacing of the moons follows an iterative scheme commonly used for studies of
compact planetary systems around single stars. For 3-moons system, we generate
MEGNO maps to calculate periodic and chaotic regions and to identify the
destabilizing MMRs. Our calculations show that the maximum number of moons
depends on the assumed masses of the satellites (Ceres-, Pluto-, and Luna-mass)
that could maintain stable orbits in a tightly-packed environment. Through our
N-body simulations, we find stable configurations for up to 7 $\pm$ 1
Ceres-mass, 4 $\pm$ 1 Pluto-mass, and 3 $\pm$ 1 Luna-mass moons. However,
outward tidal migration will likely play a substantial role in the number of
moons on stable orbits over the 10 Gyr stellar lifetime of a Sun-like star.
