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Terrestrial exoplanets in the canonical habitable zone may have a variety ofinitial water fractions due to random volatile delivery by planetesimals. Ifthe total planetary water complement is high, the entire surface may be coveredin water, forming a "waterworld." On a planet with active tectonics, competingmechanisms act to regulate the abundance of water on the surface by determiningthe partitioning of water between interior and surface. Here we explore how theincorporation of different mechanisms for the degassing and regassing of waterchanges the volatile evolution of a planet. For all of the models considered,volatile cycling reaches an approximate steady-state after $\sim 2 \\mathrm{Gyr}$. Using these steady-states, we find that if volatile cycling iseither solely dependent on temperature or seafloor pressure, exoplanets requirea high abundance ($\gtrsim 0.3\%$ of total mass) of water to have fullyinundated surfaces. However, if degassing is more dependent on seafloorpressure and regassing mainly dependent on mantle temperature, the degassingrate is relatively large at late times and a steady-state between degassing andregassing is reached with a substantial surface water fraction. If this hybridmodel is physical, super-Earths with a total water fraction similar to that ofthe Earth can become waterworlds. As a result, further understanding of theprocesses that drive volatile cycling on terrestrial planets is needed todetermine the water fraction at which they are likely to become waterworlds.

Effect of surface-mantle water exchange parameterizations on exoplanet ocean depths