  3C 84 (NGC 1275) is a well-studied mis-aligned Active Galactic Nucleus (AGN),
which has been active in Gamma rays since at least 2008. We have monitored the
source at four wavelengths (14 mm, 7 mm, 3 mm and 2 mm) using the Korean VLBI
network (KVN) since 2013 as part of the interferometric monitoring of
$\gamma$-ray bright AGN (iMOGABA) program. 3C 84 exhibits bright radio emission
both near the central supermassive black hole (SMBH) feature known as C1 and
from a moving feature located to the south known as C3. Other facilities have
also detected these short-term variations above a slowly rising trend at
shorter wavelengths, such as in Gamma ray and 1 mm total intensity
light-curves. We find that the variations in the $\gamma$ rays and 1 mm total
intensity light-curves are correlated, with the $\gamma$ rays leading and
lagging the radio emission. Analysis of the 2 mm KVN data shows that both the
Gamma rays and 1 mm total intensity short-term variations are better correlated
with the SMBH region than C3, likely placing the short-term variations in C1.
We interpret the emission as being due to the random alignment of spatially
separated emission regions. We place the slowly rising trend in C3, consistent
with previous results. Additionally, we report that since mid-2015, a large
mm-wave radio flare has been occurring in C3, with a large Gamma ray flare
coincident with the onset of this flare at all radio wavelengths.
