  The role of metallicity in shaping protoplanetary disk evolution remains
poorly comprehended. This study analyzes the disk fraction of 10 young (0.9-2.1
Myr) and low-metallicity (0.34-0.83 Z$_{\odot}$) clusters located in the outer
Milky Way with Galactocentric distances between 10 and 13 kpc. Using $JHK$ data
obtained from UKIDSS, the calculated disk fraction values for low-mass stars
(0.2-2 M$_{\odot}$) ranged from 42% to 7%. To enhance the statistical
reliability of our analysis, eight additional low-metallicity clusters are
sourced from previous studies with metallicity range 0.25-0.85 Z$_{\odot}$
along with our sample, resulting in a total of 18 regions with low-metallicity.
We find that low-metallicity clusters exhibit on average $2.6\pm0.2$ times
lower disk fraction compared to solar-metallicity clusters in all the age bins
we have. Within the age range we can probe, our study does not find evidence of
faster disk decay in sub-solar metallicity regions compared to
solar-metallicity regions. Furthermore, we observe a positive correlation
between cluster disk fraction and metallicity for two different age groups of
0.3-1.4 and 1.4-2.5 Myr. We emphasize that both cluster age and metallicity
significantly affect the fraction of stars with evidence of inner disks.
