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A key question in galaxy evolution has been the importance of the apparent`clumpiness' of high redshift galaxies. Until now, this property has beenprimarily investigated in rest-frame UV, limiting our understanding of theirrelevance. Are they short-lived or are associated with more long-lived massivestructures that are part of the underlying stellar disks? We use JWST/NIRCamimaging from CEERS to explore the connection between the presence of these`clumps' in a galaxy and its overall stellar morphology, in a mass-complete($log\,M_{*}/M_{\odot} > 10.0$) sample of galaxies at $1.0 < z < 2.0$.Exploiting the uninterrupted access to rest-frame optical and near-IR light, wesimultaneously map the clumps in galactic disks across our wavelength coverage,along with measuring the distribution of stars among their bulges and disks.Firstly, we find that the clumps are not limited to rest-frame UV and optical,but are also apparent in near-IR with $\sim 60\,\%$ spatial overlap. Thisrest-frame near-IR detection indicates that clumps would also feature in thestellar-mass distribution of the galaxy. A secondary consequence is that thesewill hence be expected to increase the dynamical friction within galactic disksleading to gas inflow. We find a strong negative correlation between how clumpya galaxy is and strength of the bulge. This firmly suggests an evolutionaryconnection, either through clumps driving bulge growth, or the bulgestabilizing the galaxy against clump formation, or a combination of the two.Finally, we find evidence of this correlation differing from rest-frame opticalto near-IR, which could suggest a combination of varying formation modes forthe clumps.

A rest-frame near-IR study of clumps in galaxies at 1 < z < 2 using JWST/NIRCam: connection to galaxy bulges