  The formation mechanism of light bridges (LBs) is strongly related to the
dynamic evolution of solar active regions (ARs). To study the relationship
between LB formation and AR evolution phases, we employ 109 LB samples from 69
ARs in 2014 using observational data from the Helioseismic and Magnetic Imager
on board the Solar Dynamics Observatory (HMI/SDO). LBs are well matched with
the weak field lanes (WFLs), except that aligned on the polarity inversion line
of {\delta} sunspots. For penumbral intrusion (type-A) and umbral-dot emergence
(type-C) LBs, the WFLs represent the splitting of magnetic flux systems. The
sunspots tend to decay and split into several parts after type-A and type-C LBs
formed. For sunspot/umbra merging (type-B) LBs, the WFLs declining are caused
by collisions of flux systems. The sunspots merge and keep stable after type-B
LBs formed. We conclude that type-B LBs are formed by collisions of flux
systems, while type-A and type-C LBs are generated by splits. The time
differences ({\delta}T) between LBs appearing and ARs peaking have average
value of 1.06, -1.60, 1.82 for type-A, B, C LBs, with the standard deviation of
3.27, 2.17, 1.89, respectively. A positive value of {\delta}T means that the LB
appear after AR peaking, whereas a minus {\delta}T before the peak. Type-A LBs
trend to form in the decaying phase or around the peak time. Type-B LBs are
more likely to be formed in the developing phase. Type-C LBs mostly take shape
in the decaying phase of ARs.
