  The recent Kepler discovery of KOI-152 reveals a system of three hot
super-Earth candidates that are in or near a 4:2:1 mean motion resonance. It is
unlikely that they formed in situ, the planets probably underwent orbital
migration during the formation and evolution process. The small semimajor axes
of the three planets suggest that migration stopped at the inner edge of the
primordial gas disk. In this paper we focus on the influence of migration
halting mechanisms, including migration "dead zones", and inner truncation by
the stellar magnetic field. We show that the stellar accretion rate, stellar
magnetic field and the speed of migration in the proto-planetary disk are the
main factors affecting the final configuration of KOI-152. Our simulations
suggest that three planets may be around a star with low star accretion rate or
with high magnetic field. On the other hand, slow type I migration, which
decreases to one tenth of the linear analysis results, favors forming the
configuration of KOI-152. Under such formation scenario, the planets in the
system are not massive enough to open gaps in the gas disk. The upper limit of
the planetary masses are estimated to be about $15,~19$, and $24 M_\oplus$,
respectively. Our results are also indicative of the near Laplacian
configurations that are quite common in planetary systems.
