  We examined the grain size in the dust ring encircling the 0.19~$M_\sun$ T
Tauri star CIDA 1 using the Karl G. Jansky Very Large Array (JVLA) at multiple
centimeter wavelengths, with a spatial resolution of 0$\farcs$2--0$\farcs$9. We
detected distinct partial-ring structures at these wavelengths around CIDA~1.
Based on spatial distributions and spectral indexes, we determined that these
centimeter emissions originated from dust, rather than free-free or synchrotron
emissions. To estimate the maximum grain size ($a_{\rm max}$) within the ring,
we compared the observed spectral energy distribution (SED) with SEDs
calculated for different $a_{\rm max}$ values using radiative transfer
calculations. Our findings indicate an $a_{\rm max}$ value of approximately
2.5~cm in the ring, assuming the dust opacity can be approximated by the DSHARP
models. These results suggest that grain growth took place within the CIDA~1
ring, potentially facilitating more efficient planet formation through pebble
accretion scenarios involving centimeter-sized pebbles.
