  The metallicity enrichment history (MEH) of a galaxy is determined by its
star formation history (SFH) and the gas cycling process. In this paper, we
construct a chemical evolution model that is regulated by the SFH of the
system. In this SFH-regulated model, the evolution of all other variables,
including the MEH, can be determined by the SFH. We test this model on six
locally isolated dwarf galaxies covering three dwarf types that were observed
by the Local Cosmology from Isolated Dwarfs (LCID) project. The SFHs and MEHs
of these LCID galaxies have been measured from the deep color-magnitude
diagrams that are down to the main sequence turn-offs stars. With simple
assumptions of the star formation law and the mass-dependent outflows, our
SFH-regulated model successfully reproduces the MEHs of all six LCID galaxies
from their SFHs, with only one free parameter, the wind efficiency $\eta \sim
1.0$, for all six galaxies. This model provides a physically motivated link
that directly connects the SFH and MEH of a galaxy, which will be useful to
accommodate into the state-of-the-art stellar population synthesis models to
help relieve the nuisance of the heavy degeneracy between the ages and
metallicities of the stellar populations.
