  Green Pea galaxies are compact galaxies with high star formation rates.
However, limited samples of Green Pea galaxies have HI 21 cm measurements.
Whether the HI gas fraction f_{HI} = M_{HI}/M_{*} of Green Pea galaxies follows
the existing scaling relations between the f_{HI} and NUV-r color or linear
combinations of color and other physical quantities needs checking. Using
archival data of HI 21cm observations, we investigate the scaling relation of
the NUV-r color with the M_{HI}/M_{*} of 38 Green Pea galaxies, including 17
detections and 21 non-detections. The HI to stellar mass ratios (f_{HI}) of
Green Pea galaxies deviate from the polynomial form, where a higher HI gas
fraction is predicted given the current NUV-r color, even with the emission
lines removed. The blue sources (NUV-r<1) from the comparison sample
(ALFALFA-SDSS) follow a similar trend. The HI gas fraction scaling relations
with linear combination forms of -0.34(NUV-r) - 0.64 log(mu_{*,z}) + 5.94 and
-0.77 log mu_{*,i} + 0.26 log SFR/M_{*}+8.53, better predict the HI gas
fraction of the Green Pea galaxies. In order to obtain accurate linear combined
forms, higher-resolution photometry from space-based telescopes is needed.
