The initial gravitational frequency is just determined from the initial orbital parameters (masses and separations) that are given in the table that comes up when you follow the link you provided. These give an initial orbital frequency (given roughly by Kepler's third law for binaries which are reasonably well separated to begin with), and for gravitational waves that depend on the acceleration of the square of the quadrupole mass moment, this means, that for circular orbits, the gravitational wave frequency is twice the orbital frequency.

Binary compact objects that have orbital frequencies high enough to be detected by aLIGO are expected to have circularised. The timescale for circularisation is shorter than the timescale on which the orbital separation changes. However, it is possible that mergers triggered by three-body interactions might lead to eccentric binary GW sources (Lower et al. 2018).

Eccentric binaries have a more complex waveform, with additional significant contributions at the orbital frequency and three times the orbital frequency. The waveform would also depend on the orientation of the orbit as we see it. Some mathematics and examples are shown in Martel & Poisson (1999).

The initial gravitational frequency is just determined from the initial orbital parameters (masses and separations) that are given in the table that comes up when you follow the link you provided. These give an initial orbital frequency (given roughly by Kepler's third law for binaries which are reasonably well separated to begin with), and for gravitational waves that depend on the acceleration of the square of the quadrupole mass moment, this means, that for circular orbits, the gravitational wave frequency is twice the orbital frequency.

Binary compact objects that have orbital frequencies high enough to be detected by aLIGO are expected to have circularised. The timescale for circularisation is shorter than the timescale on which the orbital separation changes. However, it is possible that mergers triggered by three-body interactions might lead to eccentric binary GW sources (Lower et al. 2018).

Eccentric binaries have a more complex waveform, with additional significant contributions at the orbital frequency and three times the orbital frequency. The waveform would also depend on the orientation of the orbit as we see it. Some mathematics and examples are shown in Martel & Poisson (1999).

Compact binaries with significant component spins and/or misalignment of their spin and orbital angular momentum will also produce (small) harmonics of the orbital frequency (e.g. Arun et al. 2009.

The site you link to contains a catalogue of different waveforms calculated using a numerical scheme. The calculations are complex and consumes lot of computing resources. Each calculation is followed over some tens of cycles prior to the binary merger. What determines the starting point is I think just restricting the simulation to frequencies that are in the relevant sensitivity window of GW detectors.

On the off-chance that this answers your question and while awaiting clarification.

The initial gravitational frequency is just determined from the initial orbital parameters (masses and separations) that are given in the table that comes up when you follow the link you provided. These give an initial orbital frequency (given roughly by Kepler's third law for binaries which are reasonably well separated to begin with), and for gravitational waves that depend on the acceleration of the square of the quadrupole mass moment, this means the gravitational wave frequency is twice the orbital frequency.

The initial gravitational frequency is just determined from the initial orbital parameters (masses and separations) that are given in the table that comes up when you follow the link you provided. These give an initial orbital frequency (given roughly by Kepler's third law for binaries which are reasonably well separated to begin with), and for gravitational waves that depend on the acceleration of the square of the quadrupole mass moment, this means, that for circular orbits, the gravitational wave frequency is twice the orbital frequency.

Binary compact objects that have orbital frequencies high enough to be detected by aLIGO are expected to have circularised. The timescale for circularisation is shorter than the timescale on which the orbital separation changes. However, it is possible that mergers triggered by three-body interactions might lead to eccentric binary GW sources (Lower et al. 2018).

Eccentric binaries have a more complex waveform, with additional significant contributions at the orbital frequency and three times the orbital frequency. The waveform would also depend on the orientation of the orbit as we see it. Some mathematics and examples are shown in Martel & Poisson (1999).