  We have used public JWST/NIRSpec and JWST/NIRCam observations from the CEERS
and JADES surveys in order to analyze the star-forming main sequence (SFMS)
over the redshift range $1.4 \leq z < 7$. We calculate the star-formation rates
(SFRs) of the galaxy sample using three approaches: Balmer line luminosity,
spectral energy distribution (SED) fitting, and UV luminosity. We find a larger
degree of scatter about the SFMS using the Balmer-based SFRs compared to the
UV-based SFRs. Because these SFR indicators are sensitive to star formation on
different time scales, the difference in scatter may be evidence of bursty
star-formation histories in the early universe. We additionally compare the
H$\alpha$-to-UV luminosity ratio (L(H$\alpha$)/$\nu$L$_{\nu,1600}$) for
individual galaxies in the sample and find that 29\%$-$52\% of the ratios
across the sample are poorly described by predictions from a smooth
star-formation history. Measuring the burstiness of star formation in the early
universe has multiple significant implications, such as deriving accurate
physical parameters from SED fitting, explaining the evolution of the UV
luminosity function, and providing constraints for sub-grid models of feedback
in simulations of galaxy formation and evolution.
