3C 84 (NGC 1275) is a well-studied misaligned sctive galactic nucleus (AGN), which hasbeen active in γ-rays since at least 2008. We have monitored the source at four wavelengths(14, 7, 3, and 2 mm) using the Korean VLBI network (KVN) since 2013 as part of theinterferometric monitoring of γ-ray bright AGN (iMOGABA) programme, and it exhibitsbright radio emission both near the central SMBH and in a slowly moving feature located tothe south known as C3. Other facilities have also detected these short-term variations abovea slowly rising trend at shorter wavelengths, such as in γ-ray and 1-mm total intensity lightcurves. We find that the variations in the γ -rays and 1-mm total intensity light curves arecorrelated, with the γ-ray leading and lagging the radio emission. Analysis of the 2-mmKVN data shows that both the γ-rays and 1-mm total intensity short-term variations are bettercorrelated with the SMBH region than C3, likely placing the short-term variations in C1. Weinterpret the emission as being due to the random alignment of spatially separated emissionregions. We place the slowly rising trend in C3, consistent with previous results. Spectralanalysis of the γ-ray data shows that the γ-ray flaring is inconsistent with blazar-like γ -rayemission. Additionally, we report that since mid-2015, a large mm-wave radio flare has beenoccurring in C3, with a large γ-ray flare coincident with the onset of this flare at all radiowavelengths.