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We report on the discovery of two low-luminosity, broad-line AGN at $z>5$identified using JWST NIRSpec spectroscopy from the CEERS Survey. We detectbroad H$\alpha$ emission from both sources, with FWHM of $2038\pm286$ and$1807\pm207$ km s$^{-1}$, resulting in black hole (BH) masses that are 1-2 dexbelow that of existing samples of luminous quasars at $z>5$. The first source,CEERS 1670 at $z=5.242$, is 2-3 dex fainter than known quasars at similarredshifts and was previously identified as a candidate low-luminosity AGN basedon its rest-frame optical SED. We measure a BH mass of $M_{\rmBH}=1.3\pm0.4\times 10^{7}~M_{\odot}$, confirming that this AGN is powered bythe least-massive BH known in the universe at the end of cosmic reionization.The second source, CEERS 3210 at $z=5.624$, is inferred to be a heavilyobscured, broad-line AGN caught in a transition phase between a dust-obscuredstarburst and an unobscured quasar. We estimate its BH mass to be $M_{\rmBH}\simeq 0.9-4.7 \times 10^{7}~M_{\odot}$, depending on the level of dustobscuration assumed. We derive host stellar masses, $M_\star$, allowing us toplace constraints on the BH-galaxy mass relationship in the lowest mass rangeyet probed in the early universe. The $M_{\rm BH}/M_\star$ ratio for CEERS1670, in particular, is consistent with or higher than the empiricalrelationship seen in massive galaxies at $z=0$. We examine the emission-lineratios of both sources and find that their location on the BPT and OHNOdiagrams is consistent with model predictions for low-metallicity AGN with$Z/Z_\odot \simeq 0.2-0.4$. The spectroscopic identification of low-luminosity,broad-line AGN at $z>5$ with $M_{\rm BH}\simeq 10^{7}~M_{\odot}$ demonstratesthe capability of JWST to push BH masses closer to the range predicted for theBH seed population and provides a unique opportunity to study the early stagesof BH-galaxy assembly.

Hidden Little Monsters: Spectroscopic Identification of Low-Mass, Broad-Line AGN at $z>5$ with CEERS