Dwarf stars are believed to have small protostar disk where planets may grow up .
During the planet formation stage , embryos undergoing type I migration are expected to be stalled at inner edge of magnetic inactive disk ( a _ { crit } \sim 0.2 - 0.3 ~ { } AU ) .
This mechanism makes the location around a _ { crit } a sweet spot of forming planets .
Especially , a _ { crit } of dwarf stars with masses \sim 0.5 ~ { } M _ { \odot } is roughly inside the habitable zone of the system .
In this paper we study the formation of habitable planets due to this mechanism with a model system OGLE-06-109L .
It has a 0.51 ~ { } M _ { \odot } dwarf star with two giant planets in 2.3 and 4.6 AU observed by microlensing .
We model the embryos undergoing type I migration in the gas disk with a constant disk accretion rate ( \dot { M } ) .
Giant planets in outside orbits affect the formation of habitable planets through secular perturbations at the early stage and secular resonance at the later stage .
We find that the existence and the masses of the habitable planets in OGLE-06-10L system depend on both \dot { M } and the speed of type I migration .
If planets formed earlier so that \dot { M } is larger ( \sim 10 ^ { -7 } M _ { \odot } yr ^ { -1 } ) , terrestrial planet can not be survived unless the type I migration rate is an order of magnitude less .
If planets formed later so that \dot { M } is smaller ( \sim 10 ^ { -8 } M _ { \odot } yr ^ { -1 } ) , single and high mass terrestrial planets with high water contents ( \sim 5 \% ) will be formed by inward migration of outer planet cores .
A slower speed migration will result in several planets by collisions of embryos , thus their water contents are low ( \sim 2 \% ) .
Mean motion resonances or apsidal resonances among planets may be observed if multiple planets survived in the inner system .