The gravitational wave (GW) background produced at the cosmological chiral phase transition in a conformal extension of the standard model is studied. To obtain the bounce solution of coupled field equations we implement an iterative method. We find that the corresponding O(3) symmetric Euclidean action S 3 divided by the temperature T has a simple behavior near the critical temperaturewhich is subsequently used to determine the transition's inverse duration β normalized to the Hubble parameter H. It turns out that β/H > ∼ 10 3 , implying that the sound wave period τ sw as an active GW source, too, can be much shorter than the Hubble time. We therefore compute τ sw H and use it as the reduction factor for the sound wave contribution. The signal-to-noise ratio (SNR) for Deci-Hertz Interferometer Gravitational Wave Observatory (DECIGO) and Big Bang Observer (BBO) is evaluated, with the result: SNR DECIGO < ∼ 1.2 and SNR BBO < ∼ 12.0 for five years observation, from which we conclude that the GW signal predicted by the model in the optimistic case could be detected at BBO. 1 The crossover transition in the real QCD can influence the spectrum of the inflationary GW [36-40]. The frequency band of the damped GWs is what has been predicted by Witten [33]. 2 The GWs produced during a cosmological first-oder PT in classically scale invariant models have been recently studied in refs. [44-56].